Contents

Overview

This section of the casa guide continues from the last step of the calibration one. If you completed the calibration section, then you already have the final calibrated dataset. If you just started to work on this IRAS16293 B9 data, you can download the fully calibrated dataset IRAS16293_Band9_CalibratedMS from

This casa guide covers imaging of both continuum and line of IRAS16293 Band 9. The commands in this guide should be executed in CASA 3.4.0 since CASA 3.3.0 would be very slow for the cleaning process of a big dataset like this one for IRAS16293 Band 9.
In this casa guide you will also need the Analysis Utils package, so make sure you have it imported into CASA.

Before we start with the imaging itself, do a listobs to the calibrated dataset, so you can check that everything is ok.

Continuum Emission Imaging

As it is shown in Figures 2 of IRAS16293Band9, these observations have a 7 pointing mosaic, which you can visualize with the next command (see also Figure 1).

Fig. 1. Pointings showing the mosaic used for the observations.

# Make a plot of the mosaic pattern with field ids identifiedaU.plotMosaic(vis='IRAS16293_Band9.ms',sourceid='0',doplot=True,figfile='mosaic_pattern.png')

You might wander what of these pointings or fields have stronger line emission. You can know this by running the next command. We set spw='1' containing CO (6-5), and you can check all the plots for all the fields by just hitting the arrow for "next". Also see Figure 2 for an example of the output.

Fig. 2. UV-amp distribution for the field 0 (spw 1) in the mosaic.

# See which mosaic fields have the brightest line emissionplotms(vis='IRAS16293_Band9.ms',field='',xaxis='uvdist',yaxis='amp',spw='1',avgchannel='3840',coloraxis='field',iteraxis='field')

Another way to visualize the uv-amp distribution is with the next plotms. This will load all the fields or pointing into the plot, and you can change interactively between the spws using the appropriate button in plotms. See Figure 3 for a plot of spw 0.

Fig. 3. UV-amp distribution for spw 0 using all the fields or pointings in the mosaic.

# Iterate over spws all fieldsplotms(vis='IRAS16293_Band9.ms',field='',xaxis='uvdist',yaxis='amp',spw='',avgchannel='3840',coloraxis='field',iteraxis='spw')

We need to note the channels that do not present line emission. To identify them we can plot the amplitude vs frequency for all the spectral windows. Figure 4 shows the output from the next command for spw 0 (field 3).

Fig. 4. Frequency-amplitude plot for spw 1 using the field 3. No apparent line emission is seen.

Using the plots from the previous command you can select the line emission free channels just by looking for strong lines. To do this in the rigorous way, you would need to make dirty images and then select the continuum channels.
Here we provide you with the channel selection we used for continuum emission.

The next flagmanager command will save the flags state in case you might need to re-do the steps from this point.

Clean and self-cal the continuum

Now we proceed with the cleaning itself. For the clean task you will need to choose the right cell size, map size, etc. Below are the parameters that were used in this casaguide. Note that the command will be interactive and you will have to set the cleaning boxes.

It is important to check if all fields have some emission in the model data column, if not, or very weak you would want to exclude from the gaincal below. Because the bright Source B is in all the sidelobes all fields, do have some model data components. In Figure 5 you can see an example for the output from next command.

Fig. 5. Time-amplitude plot for field 2. All spw are plotted.

# checking the model data for all the fieldsplotms(vis='IRAS16293_Band9_CONT.msAVG',xaxis='time',yaxis='amp',field='',iteraxis='field',spw='',avgchannel='4000',coloraxis='field',ydatacolumn='model',xselfscale=True,yselfscale=True)

Now we proceed with gaincal to perform self calibration (for phases) on the data. Even with minsnr=3.0 there will be failed solutions.

# get one scan per fieldos.system('rm -rf cont_pcal1')gaincal(vis='IRAS16293_Band9_CONT.msAVG',caltable='cont_pcal1',gaintype='T',refant='DV14',calmode='p',combine='',spw='',field='',solint='inf',minsnr=3.0,minblperant=4)

The solutions for five antennas are shown in Figure 6, and are produced with the next plotcal. Be sure to check all the antennas.

Fig. 6. Phase solutions for the first self-cal run.

plotcal(caltable='cont_pcal1',xaxis='time',yaxis='phase',spw='',iteration='antenna',subplot=511,plotrange=[0,0,-80,80],antenna='',timerange='')# The phases are remarkably stable for Band 9!

We then apply the table to the data to proceed right after with the proper cleaning, to check the improvement of the data.

# application of the tableapplycal(vis='IRAS16293_Band9_CONT.msAVG',spwmap=[],spw='',gaintable=['cont_pcal1'],calwt=F,flagbackup=F)

Now you are ready for the second cleaning. For this one we are using the mask resulting from the previous cleaning. In the next blocks of commands we will repeat this process (clean, viewer, gaincal, plotcal, applycal, clean, etc) to improve the overall quality of the image.

# second self-calos.system('rm -rf cont_pcal2')gaincal(vis='IRAS16293_Band9_CONT.msAVG',caltable='cont_pcal2',gaintype='T',refant='DV14',calmode='p',combine='',spw='',field='',solint='inf',minsnr=3.0,minblperant=4)#Checking the tableplotcal(caltable='cont_pcal2',xaxis='time',yaxis='phase',spw='',iteration='antenna',subplot=511,plotrange=[0,0,-80,80],antenna='',timerange='')# Applying results to the dataapplycal(vis='IRAS16293_Band9_CONT.msAVG',spwmap=[],spw='',gaintable=['cont_pcal2'],calwt=F,flagbackup=F)

We continue with the next cleaning.

os.system('rm -rf *CONTIN_P2*')clean(vis='IRAS16293_Band9_CONT.msAVG',imagename='IRAS16293_Band9.CONTIN_P2',spw='0~3',field='',phasecenter='3',mode='mfs',imagermode='mosaic',imsize=500,cell='0.04arcsec',minpb=0.25,interactive=T,weighting='briggs',robust=0.5,mask='IRAS16293_Band9.CONTIN.mask',niter=10000,threshold='0.3mJy')# to view the resulting imageimview(raster=[{'file':'IRAS16293_Band9.CONTIN_P1.image','range':[-0.01,0.5]},{'file':'IRAS16293_Band9.CONTIN_P2.image','range':[-0.01,0.5]}])# There is very little change, the bold could try another iteration using a shorter# solint phase self-cal. For now, moving on to amplitude.

Next iteration with gaincal, now using amplitude and phase for "calmode".

# For amplitude self-cal we only want to get one solution per spw, per datasetos.system('rm -rf cont_apcal')gaincal(vis='IRAS16293_Band9_CONT.msAVG',caltable='cont_apcal',gaintype='T',refant='DV14',calmode='ap',combine='scan,field',spw='',field='',solint='8000s',minsnr=3.0,minblperant=4,gaintable='cont_pcal2')# ploting the tableplotcal(caltable='cont_apcal',xaxis='time',yaxis='amp',spw='',iteration='antenna',subplot=511,plotrange=[0,0,0.5,2],antenna='',timerange='')# and applying to the dataapplycal(vis='IRAS16293_Band9_CONT.msAVG',spwmap=[],spw='',gaintable=['cont_pcal2','cont_apcal'],calwt=F,flagbackup=F)# A large correction is present for the 2nd dataset. This amplitude# error was causing many of the artifacts noticeable in the previous# images.

Continuing the the proper cleaning step.

# new cleaning for self-cal using calmode='ap'os.system('rm -rf *CONTIN_AP*')clean(vis='IRAS16293_Band9_CONT.msAVG',imagename='IRAS16293_Band9.CONTIN_AP',spw='0~3',field='',phasecenter='3',mode='mfs',imagermode='mosaic',imsize=500,cell='0.04arcsec',minpb=0.25,interactive=T,weighting='briggs',robust=0.5,mask='IRAS16293_Band9.CONTIN_P2.mask',niter=10000,threshold='0.3mJy')# and to view the imageimview(raster=[{'file':'IRAS16293_Band9.CONTIN_P2.image','range':[-0.01,0.5]},{'file':'IRAS16293_Band9.CONTIN_AP.image','range':[-0.01,0.5]}])

# correting for primary beamimpbcor(imagename='IRAS16293_Band9.CONTIN_AP.image',pbimage='IRAS16293_Band9.CONTIN_AP.flux',outfile='IRAS16293_Band9.CONTIN_AP.image.pbcor.subim',box='120,104,315,299')# and checking the imageimview(raster=[{'file':'IRAS16293_Band9.CONTIN_AP.image','range':[-0.01,0.5]},{'file':'IRAS16293_Band9.CONTIN_AP.image.pbcor.subim','range':[-0.01,0.5]}])

In Figure 6 we show the final image of all this process. The rms noise measured is about 18 mJy/beam, the restoring beam resulted in 0.236864 x 0.171968 arcsec, PA=104.419 deg. The peak values for the two components are 2.6 and 0.7 Jy, while its fluxes are 10 and 6.8 Jy.

Fig. 6. Continuum image resulted from the complete process of self calibration for the mosaic of IRAS16293 Band 9.

Now you can export your final image in fits format, so you can analyze it anytime.

Spectral Lines Imaging

Before we commence with the cleaning we need to apply the tables we produced in the self calibration steps.

# Apply final self-calibration to the line dataapplycal(vis='IRAS16293_Band9.ms.contsub',spwmap=[],spw='',gaintable=['cont_pcal2','cont_apcal'],calwt=F,flagbackup=F)

To make your work more effective we recommend you to clean cubes 1/2 spw at a time to make the image cubes a manageable size. Also, average every 2 channels since this is the native velocity resolution.

Some notes for this sections: the threshold was chosen after doing a couple of smaller test images. This is
about 3 sigma in channels with weak line emission. The mask was also chosen from a few test images. With this set, there is no need to do an interactive cleaning process.